Richard Arenstorf (1929–2014) discovered a stable periodic orbit between the Earth and the Moon which was used as the basis for the Apollo missions.
His orbit is a special case of the three body problem where two bodies are orbiting in a plane, i.
e.
the Earth and the Moon, along with a third body of negligible mass relative to the other bodies, i.
e.
the satellite.
The system of differential equations for the Arenstorf orbit are where Here the Earth is at the origin and the Moon is initially at (0, 1).
The mass of the Moon is μ = 0.
012277471 and the mass of the Earth is μ’ = 1-μ.
The initial conditions are Here’s a plot of the orbit.
I found the equations above in [1].
Richard Arenstorf I was fortunate to do my postdoc at Vanderbilt before Arenstorf retired and was able to sit in on an introductory course he taught on orbital mechanics.
His presentation was leisurely and remarkably clear.
His course was old-school “hard analysis,” much more concrete than the abstract “soft analysis” I had studied in graduate school.
He struck me as a 19th century mathematician transported to the 20th century.
He scoffed at merely measurable functions.
“Have you ever seen a function that wasn’t analytic?” This would have been heresy at my alma mater.
When I asked him about “Arenstorf’s theorem” from a recently published book I was reading, he said that he didn’t recognize it.
I forget now how it was stated, maybe involving Banach spaces and/or manifolds.
Arenstorf was much more concrete.
He wanted to help put a man on the Moon, not see how abstractly he could state his results.
More orbital mechanics posts Small course corrections Kepler and the contraction mapping theorem Orbital resonance in Neptune’s moons [1] Hairer, Nørsett, and Wanner.
Solving Ordinary Differential Equations I: Nonstiff Problems.
Springer-Verlag 1987.
.